In astrophysical reality, the evolution and properties of magnetic fields are determined by both
the dynamo growth and diffusion of magnetic fields.
Given drastically different conditions of astrophysical systems,
the turbulence parameters (e.g., driving scale, injected turbulent velocity)
and plasma parameters (e.g., magnetic Prandtl number, which is the ratio of viscosity to
magnetic diffusivity (proportional to resistivity),
ionization fraction)
for describing the dynamo and diffusion processes
can differ by many orders of magnitude between various systems
[1]}.
By contrast, numerical simulations of turbulent dynamo only cover a small range of turbulence and plasma parameters
due to the limited numerical resolution
[2]}.
Therefore, it is necessary to develop theories of turbulent dynamo applicable to
different physical regimes and astrophysical conditions,
which can also provide the recipe of the
subgrid dynamo physics for large-scale simulations
[3]}.
